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首页> 外文期刊>The Astrophysical journal >Chandra observation of diffuse gas and low-mass X-ray binaries in the elliptical galaxy NGC 4649 (M60)
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Chandra observation of diffuse gas and low-mass X-ray binaries in the elliptical galaxy NGC 4649 (M60)

机译：Chandra观测椭圆星系NGC 4649（M60）中的扩散气体和低质量X射线双星

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We present a Chandra X-ray observation of the X-ray bright E2 elliptical galaxy NGC 4649. In addition to bright diffuse emission, we resolve 165 discrete sources, most of which are presumably low-mass X-ray binaries. As found in previous studies, the luminosity function of the resolved sources is well-fitted by a broken power law. In NGC 4697 and NGC 1553, the break luminosity was comparable to the Eddington luminosity of a 1.4 M-. neutron star. One possible interpretation of this result is that those sources with luminosities above the break are accreting black holes and those below are mainly accreting neutron stars. The total X-ray spectrum of the resolved sources is well fitted by a hard power law, while the diffuse spectrum requires a hard and a soft component, presumably due to the relatively soft diffuse gas and the harder unresolved sources. We also find evidence for structure in the diffuse emission near the center of NGC 4649. Specifically, there appear to be bright "fingers'' of emission extending from the center of the galaxy and a 500 long bar at the center of the galaxy. The fingers are morphologically similar to radial features seen in two-dimensional hydrodynamic simulations of cooling flows in elliptical galaxies, and although their other properties do not match the predictions of the particular simulations used, we conclude that the radial fingers might be due to convective motions of hot outflowing gas and cooler inflowing gas. The bar is coincident with the central extended radio source; we conclude that the bar may be caused by weak shocks in the diffuse gas from an undetected low-luminosity active galactic nucleus. [References: 31]
机译：我们对X射线明亮的E2椭圆星系NGC 4649进行Chandra X射线观察。除了明亮的漫射发射，我们还解析了165个离散源，其中大多数可能是低质量X射线双星。如先前的研究中所发现的那样，已分解光源的光度函数很适合被打破的幂定律。在NGC 4697和NGC 1553中，断裂光度与1.4 M-的爱丁顿光度相当。中子星。对此结果的一种可能解释是，那些具有高于断裂的光度的源正在吸收黑洞，而那些低于其光度的源则主要在吸收中子星。解析源的总X射线光谱通过硬幂定律很好地拟合，而扩散谱需要硬和软成分，这大概是由于相对较软的扩散气体和较硬的未解析源。我们还在NGC 4649中心附近的漫射中找到结构的证据。特别是，似乎有明亮的发射“指状物”从银河系中心延伸，在银河系中心有500长条。指形在形态上类似于椭圆星系中冷却流的二维水动力模拟中看到的径向特征，尽管它们的其他属性与所使用的特定模拟的预测不匹配，但我们得出的结论是，指形可能是由于对流运动造成的。热棒流出的气体和较冷的流入气体的棒与中央扩展无线电源重合；我们得出的结论是，棒可能是由于未检测到的低发光活性银河核引起的扩散气体中的弱震动引起的[参考文献：31]

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